Lecture 8: Interconnecton

Departm

ent of Physics and A

stronomy

Texas A&

M U

niversity &

D

epartment of P

hysics K

yungpook National U

niversity

1

1

http://faculty.physics.tamu.edu/kam

on/teaching/phys824wcu/ 22

So fa

r …

Lec 0: IceCube (HW

01) Lec 1: Introduction – PPC, H

iggs and SUSY

Lec 2: Higgs M

echanism

Lec 3: Higgs production and decay at the LH

C Lec 4: H

iggs searches at CMS

Lec 5: Collider detectors (and CMS)

Lec 6: CMS ECA

L Lec 7: Lec 6 Review (H

W 02)

RRe

ca

ps

3

HHig

gs M

ec

ha

nism

4

Closer look …

The illustration is not accurate.

HHig

gs In

tera

ctio

n

5

Electron field M

uon field

Muon field

Electron field

Electromagnetic field + electron field [propagation of EM

force

Higgs field’s vacuum

expectation is non-zero everywhere in the universe. �

Higgs field

can “interact” with particle fields. �

Gives masses to all other particles (ferm

ions)

gFundam

ental Interaction

We

have

ob

serve

d a

ne

w b

oso

n

with

a m

ass o

f 1

25

.3 ±

0.6

Ge

V at 4

.9 � !

Re

ca

p: C

MS

Hig

gs S

um

ma

ry

[GeV]

4lm

Events / 3 GeV

0 2 4 6 8 10 12

[GeV]

4lm

Events / 3 GeV

0 2 4 6 8 10 12Data

Z+X*,ZZ�Z=126 G

eVH

m

�, 2e2�

7 TeV 4e, 4�

, 2e2�

8 TeV 4e, 4

CMS Prelim

inary-1

= 8 TeV, L = 5.26 fbs

; -1

= 7 TeV, L = 5.05 fbs

[GeV]

4lm

80100

120140

160180 �e2�e2V] 80

6

���

H)

)((

ZZH

*��

���

�p

-valu

e

KKey D

ete

cto

r Syste

m fo

r H�

���

7

Ele

ctro

ma

gn

etic

Ca

lorim

ete

r (EC

AL

)

���

H��

�H

Hig

h e

ne

rgy re

solu

tion

F

ine

seg

me

ntatio

n

Lo

w e

ne

rgy re

solu

tion

C

oarse se

gm

en

tation

Le

t’s che

ck EC

AL

…

Illustrative

p

urp

ose

K. N

akamura et al. (Particle D

ata Group), J. Phys. G

37, 075021 (2010)

RRe

ca

p: E

lec

trom

ag

ne

tic C

asc

ad

e

)(

)(

1

0a e

btb

Edt dE

bta�

��

�

b atmax

1at

�

[No

te] a

diffe

ren

ce

be

twe

en

e a

nd

��

20 X0 is a pretty good thickness.

8

1.5 X0 C

ubic

Full Size Samples

Belle C

sI(Tl): 16 X0

L3 BG

O: 22 X

0 C

MS PW

O: 25 X

0

Belle C

sI(Tl)

L3 BG

O

CM

S PWO

(Y)

PbWO

4

BG

O

CeF

3

BaF

2 C

sI B

aFC

sI

CCrysta

l Sc

intilla

tors

9

QQu

estio

ns

EC

AL’s RR

eeqq

uuiirree

mmee

nnttss

High energy resolution & fast response?

� Tech

no

log

ies?

Fine granularity? � O

f ord

er o

f latera

l sho

we

r size – fin

d a

typic

allate

ral sp

rea

d o

f EM

sho

we

rs � T

he

ea

ch to

we

r size is o

f ord

er o

f the

latera

l sho

we

r wh

ich is sm

all e

no

ug

h to

m

inim

ize a

n o

verla

p w

ith o

the

r pa

rticles fro

m p

ile-u

p in

tera

ctio

ns.

Uniform

ity? � C

alib

ration

Radiation H

ard? � L

imite

d life

time

10

CCa

libra

tion

11

Medical application

Nondestructive analysis

High energy physics

Security check

Board inspection

Radiation m

onitoring

Astro-particle physics, ....

X-ray scanning

Scintillation Detectors

Scintillation Surveymeter

NaI(Tl) Spectrom

eter

Ap

plic

ation

s of S

cin

tillators

12

Inn

er T

racke

r Syste

m

Pixel detector starts at ~ 4cm

Outer silicon tracker ends at ~ 1m

Tracks the trajectory of charged particles

Ele

ctro

ma

gn

etic

Ca

lorim

ete

r (EC

AL)

Lead Tungstate crystals

Designed to detect e’s and �’s

H

ad

ron

Ca

lorim

ete

r (HC

AL

) B

rass and steel material sam

pled in with

scintillators D

esigned to detect hadrons

So

len

oid

Ma

gn

et

3.8 T strength for the precise m

easurement of particle m

omentum

Mu

on

De

tec

tor

Syste

mG

as detectors

Inra

cker

Syste

mT

re

rT

ne

CM

S D

ete

cto

r –S

om

e D

eta

ils

13

CCa

lorim

ete

r “Tow

er” G

eo

me

try

= 0.696

= 2.704

A design to m

easure the direction of energy flow

�

�

�k

Ej

Ei

EE

cos

sin

sin

cos

sin

tow

ertow

ertow

ertow

er�

�

�

��

��

�� ��� �

�� ��� �

��

2tan

ln�

Forw

ard

Ca

lorim

ete

r, n

ot sh

ow

n

= 0

��

14

η

Barrel (R

ef : DN

-2010/021)

Specification Total

Gap(inter-crytal)

0.5 mm

Crack(inter-

supercrystal) 2.2 m

m

Endcap(Ref : D

N-2010/005)

25x20 20x20

20x20 20x20

0.0 0.44

0.79 1.14

1.479 1.6

2.6

Crack

+M1

+M2

+M3

+M4

-M3

-M2

-M1

-M4

EC

AL

“Tow

er” G

eo

me

try

15

AAT

LA

S vs. C

MS

ma

gn

et

Note: the difference in its detector configurations

16

CCo

llide

r De

tec

tors

ATLAS

CM

S C

DF II

D0 II

Magnetic

field 2 T solenoid + toroid (0.5 T barrel 1 T endcap)

4 T solenoid + return yoke

1.4T solenoid 2T solenoid + toroid (1.8T)

Tracker Si pixels, strips + TR

T σ/p

T ≈ 5x10-4 p

T + 0.01

Si pixels, strips σ/p

T ≈ 1.5x10-4 p

T + 0.005

Si strips + drift cham

ber Si strips + scintillating fiber

EM

calorimeter

Pb+LAr σ/E ≈ 10%

/√E + 0.007

PbWO

4 crystals σ/E ≈ 3%

/√E � 0.003

Pb+scintillator σ/E ≈ 13.5%

/√E �

0.015 in barrel

U+LAr

Hadronic

calorimeter

Fe+scint. / Cu+LAr

(10λ) σ/E ≈ 50%

/√E �

0.03

Brass+scintillator (7

λ + catcher) σ/E ≈ 100%

/√E �

0.05

Iron+scintillator σ/E ≈ 50%

/√E � 0.03

in barrel

U+LAr (C

u or stainless in outer hadronic)

Muon

σ/pT ≈ 2%

@ 50G

eV to 10%

@ 1TeV

(ID+M

S)

σ/pT ≈ 1%

@ 50G

eV to 10%

@ 1TeV

(DT/C

SC+Tracker)

Rapidities to 1.4

Rapidities to 2.0

17

AAstro

nom

ical D

ark

Matter

18

119

Wh

o W

an

ted

“Da

rk Matte

r”?

DM

[http://en.wikipedia.org/wiki/Fritz_Zwicky] W

hile examining the Com

a Galaxy Cluster (large cluster of galaxies - over 1,000 identified galaxies; m

ean distance from Earth is 99 Mpc or 321 m

illion ly) in 1933, Zwicky was the first to use the Virial Theorem

to infer the existence of unseen matter,

what is now called Dark Matter. He was able to infer the average m

ass of galaxies within the cluster, and obtained a value about 160 tim

es greater than expected from

their luminosity, and

proposed that most of the m

atter was dark. The sam

e calculation today shows a smaller factor,

based on greater values for the mass of lum

inous m

aterial; but it is still clear that the great majority

of matter is dark.

II did

…

20

Astrophysical Journal 159 (1970) 377

Rotation curve

of a

typical spiral

galaxy: predicted (A) and observed (B). The discrepancy between the curves is attributed to dark m

atter. 22

1

Astrophysical Journal 159 (1970) 377D

ark M

atter in

Sp

iral G

ala

xy

EEvid

en

ce

for D

ark M

atte

r

22

MMo

re E

vide

nc

e fo

r Da

rk Ma

tter

23

February 9, 2008 D

ark Particle H

unters

4 3 2 1 Splitting ordinary m

atter and dark matter

– Another Clear Evidence of D

ark Matter –

(8/21/06)

Dark M

atter (G

ravitational Lensing)

Ordinary M

atter (N

ASA’s C

handra X

Observatory)

time

Approxim

ately the sam

e size as the M

ilky Way

Splittingordinary

matterand

darkmm

atterm

Dark M

atter in the Universe

24

Can it be one of the known particles? Let’s check out!

It Doesn’t M

atter. R

ight, it doesn’t shake hand with anyone easily. Tw

o dark m

atter clusters (in blue) are just passing each other. It is a long-lived (stable) object. It’s a C

old Matter.

Yes, it is a “relativistically” slow

ly moving (“cold”)

object.

4

It’s an Invisible Matter.

Right, it doesn’t respond to your flash light.

This means it is a neutral object.

So, It’s a Cold Dark M

atter (CD

M).

ItD

oesn’tM

atter

PPro

pe

rties o

f Co

ld D

ark M

atter

25

Qu

iz [[Q

] Ca

n b

e th

e d

ark m

atter a

Sta

nd

ard

Mo

de

l pa

rticle?

[Recap: Dark m

atter particles] (1)

Weakly interacting

(2)N

eutral (3)

Heavy …

relativistically slowly m

oving

[A]

Quarks,

electron, muon,

and tau

cannot be

dark matter, because they are interacting via strong and/or

electromagnetic forces. N

eutrinos are too light. [Q

] Wh

at sho

uld

we

do

?

[A] Expand the Standard M

odel framework based on a

new symmetry, e.g., Supersym

metry or SU

SY (next page)

� N

ew particles, including a dark matter candidate

26

SSu

pe

rsymm

etry (S

US

Y)

27

Fermions

Bosons

A set of new particles, including a dark m

atter candidate

Spin (&

charge) is

a fundam

ental property

and a powerful tool in inform

ation technology. See

Lecture 1

by Prof.

Sinova on

Jan. 28.

IInterco

nn

ection

28

PPa

rticle P

hysic

s an

d C

osm

olo

gy

�

8

pb

0.9

1

230

2 2

ann

0 ann

201

Mv

dxv

~h

.

fx

~

��

�

��

�

�

��

�

SU

SY

is

an

in

tere

sting

cla

ss o

f m

od

els to

pro

vide

a m

assive

ne

utra

l p

article

(M ~

10

0 G

eV

) an

d w

ea

kly in

tera

ctin

g (W

IMP

).

SUSY

CD

M =

=

Ne

utra

linoo o( ))

01� ~

Astrophysicscs

29

~0.0000001 seconds

Now

CM

B

annihilation

combination

LHC

http://ww

w.dam

tp.cam.ac.uk/user/gr/public/bb_history.htm

l

LHC D

ark

Matter a

nd S

USY

Pro

bin

g ~

10

-7 sec. a

fter B

ig B

an

g

30

�

32

2eq

nn

Hn

dt dn�

!�

��

v�

Thermal Equilibrium

Co

nn

ec

ting

Pa

rticle P

hysic

s an

d C

osm

olo

gy

Annihilation

Combination

31

DDM

An

nih

ilation

32

DDM

An

nih

ilation

+ C

om

bin

ation

33

“Num

ber” density (n) �� �

Cross section (�)

SUSY M

asses (at the LHC)

masses)

(S

US

Y2

01D

�h

~��

]M

pcs

km

100[

11

��

!"

/H

h

�

32

2eq

nn

Hn

dt dn�

!�

��

v�

2

2

� � � �� �

� � � �� �

�

� � � �� �

� � � �� �

#ann

�+ …

. + …

.

Co-annihilation (C

A) Process

(Griest, Seckel ’91)

34

PPo

ssible

Da

rk Ma

tter In

tera

ctio

ns

35

HHo

t To

pic

36

(Oct 29, 2012

) Today's High Energy Theory sem

inar will be given by H

aibo Y

u visiting from M

ichigan:

Exploring Dark M

atter From C

olliders to the Cosm

os A

strophysical and cosmological observations provide com

pelling evidence

for the existence of dark matter in the U

niverse, but its particle physics nature

remains

mysterious.

The w

eakly-interacting m

assive particle

(WIM

P) has been proposed as a dark m

atter candidate. In this talk, I w

ill first show that particle colliders including the Tevatron

and the LHC

are powerful tools to hunt for W

IMP

dark matter.

I will also discuss dark m

atter models beyond the W

IMP

paradigm and

search strategies for them. A

strophysical objects such as neutron stars and dw

arf galaxies

provide natural

laboratories for

exploring dark

matter

beyondthe

WIM

P.

Date/tim

e: October 29, 2pm

. R

oom: M

IST M102.

HHu

nt fo

r Da

rk Ma

tter

Ha

ibo

Yu

37